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Astro2020 Science White Paper Single-Object Imaging and Spectroscopy to Enhance Dark Energy Science from LSST

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Astro2020 Science White Paper Single-Object Imaging and Spectroscopy to Enhance Dark Energy Science from LSST Astro2020 Science White Paper Single-object Imaging and Spectroscopy to Enhance Dark Energy Science from LSST Thematic Areas: Cosmology and Fundamental Physics Principal (corresponding) author: Name: R. A. Hloˇzek Institution: Department of Astronomy and Astrophysics & Dunlap Institute for Astronomy and Astrophysics, University of Toronto Email: [email protected] Phone: +1 416-978-4971 Co-authors: T. Collett (IoCG, Portsmouth), L. Galbany (U. Pittsburgh, PITT PACC), D. A. Goldstein (Caltech, Hubble Fellow), S. W. Jha (Rutgers), A. G. Kim (LBNL), R. Man- delbaum (CMU), J. A. Newman (U. Pittsburgh, PITT PACC), S. Perlmutter (LBNL, UC Berkeley), D. J. Perrefort (U. Pittsburgh, PITT PACC), M. Sullivan (Southampton), and A. Verma (U. Oxford), for the LSST Dark Energy Science Collaboration Abstract: Single-object imaging and spectroscopy on telescopes with apertures ranging from ∼ 4m to 40m have the potential to greatly enhance the cosmological constraints that can be obtained from LSST. Two major cosmological probes will benefit greatly from LSST follow-up: accurate spectrophotometry for nearby and distant Type Ia supernovae will ex- pand the cosmological distance lever arm by unlocking the constraining power of high-z supernovae; and cosmology with time delays of strongly-lensed supernovae and quasars will require additional high-cadence imaging to supplement LSST, adaptive optics imaging or spectroscopy for accurate lens and source positions, and IFU or slit spectroscopy to measure detailed properties of lens systems. We highlight the scientific impact of these two science drivers, and discuss how additional resources will benefit them. For both science cases, LSST will deliver a large sample of objects over both the wide and deep fields in the LSST survey, but additional data to characterize both individual systems and overall systematics will be key to ensuring robust cosmological inference to high redshifts. Community access to large amounts of natural-seeing imaging on ∼2{4m telescopes, adaptive optics imaging and spectroscopy on 8{40m telescopes, and high-throughput single-target spectroscopy on 4{40m telescopes will be necessary for LSST time domain cosmology to reach its full potential. In two companion white papers we present the additional gains for LSST cosmology that will come from deep and from wide-field multi-object spectroscopy. 1 Introduction As a Stage IV Dark Energy program, the Large Synoptic Survey Telescope (LSST) will play a major role in improving our knowledge of cosmology over the years 2023{2033 via both wide-area and deep surveys. However, obtaining measurements that extract the full potential of LSST will require additional data from other ground-based facilities. In this white paper, we describe the science opportunities to build on and strengthen the LSST dataset that would be made possible by community access to telescopes and instruments enabling detailed follow-up of individual objects. These facilities can provide single-object imaging either in more bands, with higher spatial resolution, or with higher cadence than the LSST observations provide, and can provide spectroscopic measurements for rare objects, which are difficult to target efficiently for multi-object spectroscopy. In two companion white papers we describe the gains for LSST cosmology that would come from community access to highly-multiplexed optical and infrared spectroscopy on 4{ 40 m telescopes, either via surveys of faint objects at the full depth of LSST cosmological samples, i∼25 [1], or from wider-area (> 20deg2) but shallower surveys [2]. 2 Type Ia Supernova Spectroscopy to High Redshifts As described in a companion paper [2], the largest sets of redshift measurements for LSST supernovae should come from targeting SNe and their host galaxies via wide-field multi- object spectroscopy, either using a small fraction of fibers in surveys that span the LSST footprint or via targeted surveys in the LSST Deep Drilling Fields (DDFs). However, higher signal-to-noise observations will be needed for a significant sample of low-z SNe to charac- terize the range of intrinsic spectra; and to compare this to the high-z LSST Type Ia SN (z ∼ 0:5 − 1:4) will require targeted long-exposure follow-up while the high-z SNe are still bright. Typing to eliminate non-SNe Ia contamination and to validate photometric classification at high (and low) redshift: Much work has gone into techniques for de- termining supernova types and redshifts from photometry alone, but this is still a difficult technique when applied over a large redshift range due to changing filter coverage and un- known drifts in the spectroscopic properties of the SNe. Current photometric identification techniques require spectroscopically classified training samples, ideally over the full range of redshifts under consideration. Fully characterizing some classes of objects from LSST at the faintest magnitudes [e.g., SLSN and Type II SN, see 3; 4] will require spectroscopic observations on 25{40 m class telescopes. Furthermore, measuring the redshifts via spectra of \live" supernovae eliminates type uncertainty, yielding high-purity samples with limited systematics. Ultimately, detailed spectrophotometric studies of low-z Type Ia SN will be the best source of high-signal-to-noise information about the behavior over a large range of Type Ia SN subtypes, making spectroscopy on smaller telescopes valuable as well. An example of such a study can be found in [5]. Systematic error mitigation: Detailed understanding of a variety of potential sources of systematic error will be crucial for supernova science with LSST, including evolution of the Type Ia SN population with redshift; errors in the specification of the spectral energy 1 distribution (SED) in different redshift/rest-frame wavelength ranges that can affect training of light curve models; and mis-classifying fine sub-types (\twins") of Type Ia supernovae. Finally, we do not know if our current catalog of spectral properties is exhaustive, and, if not, the mismatch between assumed spectral model templates and actual spectra will introduce systematic shifts in our cosmological distance measurements. While deep follow- up of a variety of LSST transients will be needed to understand their physics and evolution, requirements for the use of SNe Ia as cosmic probes of distance are particularly stringent, and hence detailed spectral studies are needed. Very high data quality is needed if spectra of \live" supernovae will be used to detect the subtle differences between sub-types of SN Ia, to study evolutionary population drift, and to match highly-similar supernovae (\twins" as described in [6]) to reduce the dispersion of measured distances. So far, such purposes require high signal-to-noise observations to track subtle spectroscopic features and spectrophotometric data to allow a clean subtraction of the host galaxy light. For systematics constraints on measurements of high-redshift Type Ia SN to be commensurate with the precise statistical uncertainties resulting from large numbers of LSST-discovered SNe, there will be a need for new instrumentation for ground-based telescopes (e.g., IFU or high-throughput spectrographs now in the planning stages for 2{4 m telescopes and IFU reformatters on existing spectrographs (with or without AO) on 8{40 m telescopes), as well as development of space-based observational avenues such as coordinated observations with Euclid, WFIRST or other space missions now planning spectrophotometric instrumentation. 3 Cosmology with Strong Gravitational Lens Systems One of the most striking consequences of general relativity is that light from distant sources is deflected by the gravitational field of massive objects near the line of sight. When the deflection produces multiple images, the phenomenon is known as \strong gravitational lens- ing." The multiple images of strongly lensed sources arrive at different times because they travel different paths and through different gravitational potentials to reach us [7; 8]. When a strongly lensed source is time variable, the arrival time delays can be measured and combined with a mass model to yield cosmological constraints, particularly on the Hubble constant H0. Strongly-lensed QSOs, compound lens systems, and strongly-lensed supernovae each provide opportunities for measurement of cosmological parameters with LSST, and the LSST DESC plans to exploit them all [9]. 3.1 Precision Cosmology with Strongly-Lensed Supernova Time Delays The prospect of cosmological constraints from strongly-lensed supernovae was illustrated with the ground-breaking Hubble Space Telescope observations of the first multiply-imaged lensed supernova, SN Refsdal [10]. Ground-based time-domain optical imaging surveys sim- ilar in spirit to LSST, such as the intermediate Palomar Transient Factory (iPTF), played a key role in the discovery and follow-up observations of another strongly gravitationally lensed supernova with resolved multiple images [11, see Figure 1]. Time delays from lensed supernovae present opportunities to observe the earliest phases of supernova explosions, to infer cosmological parameters, and to map substructure in lens 2 Figure 1: iPTF16geu, a Type Ia supernova at z = 0:4 strongly lensed by an elliptical galaxy at z = 0:2 (data from HST and Keck). This transient|the only known lensed Type Ia SN with resolved multiple images|was discovered by a predecessor of LSST, the intermediate Palomar Transient Factory (iPTF). The multiple images of the supernova are indicated with circles. Due to the
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